celeries.mmr.MMR.ell2v

MMR.ell2v(ell, km_max=None)

Convert elliptical coordinates to the coordinates of the average problem v = (y, phi, x, dL).

Parameters:

ell(npla, 4,) ndarray

Astrocentric coordinates: a (semi-major axis), e (eccentricity), \(\lambda_0\) (mean longitude), and \(\varpi\) (longitude of periastron) of the planets.

km_maxint or None

If provided, the change of variables due to averaging is peformed, including terms up to km_max.

Returns:

v(4*npla-4,) ndarray

Normalized coordinates (y, phi, x, dL).

deltafloat

Value of delta (normalized by Gamma).

Gammafloat

Value of Gamma, setting the scale of the system.